Dust from collisions: A way to probe the composition of exo-planets?

摘要: In order to link infrared observations of dust formed during planet formation in debris disks mid-infrared spectroscopic data planetary materials from differentiated terrestrial and asteroidal bodies, we obtained absorption spectra a representative suite crustal mantle materials, typical martian meteorites. A series disk characterized by strong feature the 9.0–9.5 µm range (HD23514, HD15407a, HD172555 HD165014), is comparable that underwent shock, collision or high temperature events. These are amorphous such as tektites, SiO2-glass, obsidian, highly shocked shergottites well inclusions mesosiderites (group A). second group (BD+20307, Beta Pictoris, HD145263, ID8, HD113766, HD69830, P1121, Eta Corvi) have pyroxene olivine bands 9–12 very similar ultramafic rocks (e.g. harzburgite, dunite) B). This could indicate occurrence those our Solar System these other systems. However, mixing projectile target material, material has be taken into account large scale events like hit-and-run giant collisions even large-scale impacts. This explain olivine-dominated B. The crustal-type A would possibly require stripping upper layers grazingstyle hit-and run encounters energy evaporation/condensation collisions. In tidal disruptions involvement predominantly icy/water bodies resulting mineral would originate mainly one involved planetesimals. allow attributing observed composition specific body (such e.g. Corvi).